If all PBHs evaporated completely during the radiation-dominant era before BBN, the energy density of particle species \(i\)  from PBHs evaporation is obtained as [1]}
\(\Omega _i &=& 3.553 \left(\frac{\gamma }{0.2}\right)^{1/2} \left(\frac{0.67}{h}\right)^{2} \left(\frac{106.75}{g_\ast }\right)^{1/4} \nonumber \\&& \times \left(\frac{1{\rm g}}{M_{\rm PBH}}\right)^{3/2} \beta \left(\frac{m_i}{1{\rm GeV}}\right)\mathcal {N}_i,\) 
